Search for Cosmic-Ray Boosted Sub-GeV Dark Matter Using Recoil Protons at Super-Kamiokande

Abe, K.; Hayato, Y.; Hiraide, K.; Ieki, K.; Ikeda, M.; Kameda, J.; Kanemura, Y.; Kaneshima, R.; Kashiwagi, Yosuke; Kataoka, Y.; Miki, S.; Mine, S.; Miura, M.; Moriyama, S.; Nakano, Y.; Nakahata, M.; Nakayama, S.; Noguchi, Y.; Okamoto, Ken‐ichi; Sato, Kenta; Sekiya, H.; Shiba, Hayato; Shimizu, Kurakazu; Shiozawa, M.; Sonoda, Y.; Suzuki, Yoshihiro; Takeda, Atsushi; Takemoto, Y.; Takenaka, A.; Watanabe, S.; Yano, T.; Han, S.; Kajita, T.; Okumura, K.; Tashiro, T.; Tomiya, Tomoaki; Wang, X.; Xia, Jingkai; Yoshida, Shigeru; Megías, G. D.; Fernández, P.; Labarga, L.; Ospina, N.; Zaldívar, Bryan; Pointon, B. W.; Kearns, E.; Raaf, J. L.; Wan, L.; Wester, T.; Bian, J. G.; Griskevich, N. J.; Kropp, W. R.; Locke, S.; Smy, M. B.; Sobel, H. W.; Takhistov, Volodymyr; Yankelevich, A.; Hill, J.; Park, R. G.; Bodur, B.; Scholberg, K.; Walter, C. W.; Bernard, L.; Coffani, A.; Drapier, O.; Hedri, Sonia El; Giampaolo, A.; Mueller, T.; Santos, Angelo De Souza; Paganini, P.; Quilain, B.; Ishizuka, T.; Nakamura, T.; Jang, J. S.; Learned, J. G.; Choi, K.; Cao, S.; Anthony, L. H. V.; Martin, Dirk; Scott, M.; Sztuc, A. A.; Uchida, Y.; Berardi, V.; Catanesi, Maria Gabriella; Radicioni, E.; Calabria, N. F.; Machado, L. N.; Rosa, G. De; Collazuol, G.; Iacob, F.; Lamoureux, Mathieu; Mattiazzi, M.; Ludovici, L.; Gonin, M.; Pronost, G.; Fujisawa, C.; Maekawa, Y.; Nishimura, Y.; Friend, M.; Hasegawa, T.; Ishida, Toru; Kobayashi, T.; Jakkapu, M.; Matsubara, T.; Nakadaira, T.; Oyama, Y.; Sakashita, K.; Sekiguchi, T.; Tsukamoto, T.; Boschi, T.; Lodovico, F. Di; Jian, Gao; Goldsack, A.; Katori, T.; Migenda, J.; Taani, M.; Zsoldos, S.; Kotsar, Y.; Ozaki, H.; Suzuki, A.; Takeuchi, Y.; Bronner, C.; Feng, Jie-Cheng; Kikawa, T.; Mori, M.; Nakaya, T.; Wendell, R.; Yasutome, K.; Jenkins, S. J.; McCauley, N.; Mehta, Poonam; Tsui, K. M.; Fukuda, Y.; Itow, Y.; Menjo, H.; Ninomiya, Kansuke; Łagoda, J.; Lakshmi, S.; Mandal, M.; Mijakowski, P.; Prabhu, Y. S.; Zalipska, J.; Jia, M.; Jiang, Jun; Jung, C. K.; Wilking, M. J.; Yanagisawa, C.; Harada, Masayuki; Ishino, H.; Ito, S.; Kitagawa, Hiroshi; Koshio, Y.; Nakanishi, F.; Sakai, S.; Barr, G.; Barrow, D.; Cook, L.; Samani, S.; Wark, D.; Nova, F.; Yang, Jijun; Malek, M.; McElwee, J.; Stone, O.; Thiesse, M.; Thompson, L.F.; Okazawa, H.; Kim, S. B.; Seo, J. W.; Yu, I.; Ichikawa, A. K.; Nakamura, Kenzo; Tairafune, S.; Nishijima, K.; Iwamoto, K.; Nakagiri, K.; Nakajima, Yasuhiro; Taniuchi, N.; Yokoyama, M.; Martens, K.; Perio, P. de; Vagins, M. R.; Kuze, M.; Izumiyama, S.; Inomoto, M.; Ishitsuka, M.; Itô, Hiroshi; Kinoshita, T.; Matsumoto, R.; Ommura, Yuga; Shigeta, N.; Shinoki, M.; Suganuma, T.; Yamauchi, K.; Martin, J. F.; Tanaka, Hirohisa; Towstego, T.; Akutsu, R.; Gousy-Leblanc, V.; Hartz, M.; Konaka, A.; Prouse, N. W.; Chen, S.; Xu, B. D.; Zhang, B.; Posiadała-Zezula, M.; Hadley, D. R.; Nicholson, M. E.; O’Flaherty, M.; Richards, B.; Ali, Ahmed Farag; Jamieson, B.; Marti, Ll.; Minamino, A.; Pintaudi, G.; Sano, S.; Suzuki, S.; Wada, Keiichi

doi:10.1103/physrevlett.130.031802

Cited by 24 publications

(15 citation statements)

References 48 publications

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“…This analysis allows a ∼100 keV fermion mass (Yunis et al 2020). On the other hand, promising direct searches of dark matter in terrestrial laboratories, e.g., xenon, krypton, and argon detectors, via the dark matter interactions with ordinary matter, electrons, and nucleons, via kinetic energy recoils or even target ionization have started to look for a dark matter fermion in the tens of keV range (see, e.g., Dror et al 2020;Shakeri et al 2020;Dror et al 2021;Aprile et al 2022;Ge et al 2022;Li et al 2022;Zhang et al 2022;Aalbers et al 2023;Abe et al 2023;Caddell et al 2023;PandaX Collaboration et al 2023;Rebeiro et al 2023;Smirnov & Trautner 2023, and references therein). This is precisely the fermion mass-energy range that we have inferred from combined astrophysical analyses.…”

Section: Discussionmentioning

confidence: 99%

Baryon-induced Collapse of Dark Matter Cores into Supermassive Black Holes

Argüelles,

Rueda,

Ruffini

2024

ApJL

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Nonlinear structure formation for fermionic dark matter particles leads to dark matter density profiles with a degenerate compact core surrounded by a diluted halo. For a given fermion mass, the core has a critical mass that collapses into a supermassive black hole (SMBH). Galactic dynamics constraints suggest a ∼100 keV/c 2 fermion, which leads to ∼107 M ⊙ critical core mass. Here, we show that baryonic (ordinary) matter accretion drives an initially stable dark matter core to SMBH formation and determines the accreted mass threshold that induces it. Baryonic gas density ρ b and velocity v b inferred from cosmological hydrosimulations and observations produce sub-Eddington accretion rates triggering the baryon-induced collapse in less than 1 Gyr. This process produces active galactic nuclei in galaxy mergers and the high-redshift Universe. For TXS 2116–077, merging with a nearby galaxy, the observed 3 × 107 M ⊙ SMBH, for Q b = ρ b / v b 3 = 0.125 M ⊙ / ( 100 km s − 1 pc ) 3 , forms in ≈0.6 Gyr, consistent with the 0.5–2 Gyr merger timescale and younger jet. For the farthest central SMBH detected by the Chandra X-ray satellite in the z = 10.3 UHZ1 galaxy observed by the James Webb Space Telescope (JWST), the mechanism leads to a 4 × 107 M ⊙ SMBH in 87–187 Myr, starting the accretion at z = 12–15. The baryon-induced collapse can also explain the ≈107–108 M ⊙ SMBHs revealed by JWST at z ≈ 4–6. After its formation, the SMBH can grow to a few 109 M ⊙ in timescales shorter than 1 Gyr via sub-Eddington baryonic mass accretion.

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Section: Discussionmentioning

confidence: 99%

Baryon-induced Collapse of Dark Matter Cores into Supermassive Black Holes

Argüelles,

Rueda,

Ruffini

2024

ApJL

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“…Thus, the effect of the nuclear form factor for halo DM can be safely neglected. Note that for CR boosted DM the form factor may play a significant role [40,41].…”

Section: Underground Dm Distributionsmentioning

confidence: 99%

“…The constraints from XENON10 (orange dotted) and XENON1T (green dotted) [19] calculated using the QEdark code [68] and the constraints from DarkSide-50 [58] on the Migdal effect of halo DM are shown. The constraints from the data of Super-K on the cosmic-ray boosted DM are also shown for comparison [41]. The two red markers represent two benchmark parameter sets of DM particle masses and DM-nucleon scattering cross sections.…”

Section: Constraints On Dm-nucleon Scattering Cross Sectionsmentioning

confidence: 99%

Diurnal modulation of electron recoils from DM-nucleon scattering through the Migdal effect

Qiao,

Xia,

Zhou

2023

J. Cosmol. Astropart. Phys.

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Halo dark matter (DM) particles could lose energy due to the scattering off nuclei within the Earth before reaching the underground detectors of DM direct detection experiments. This Earth shielding effect can result in diurnal modulation of the DM-induced recoil event rates observed underground due to the self-rotation of the Earth. For electron recoil signals from DM-electron scatterings, the current experimental constraints are very stringent such that the diurnal modulation cannot be observed for halo DM. We propose a novel type of diurnal modulation effect: diurnal modulation in electron recoil signals induced by DM-nucleon scattering via the Migdal effect. We set so far the most stringent constraints on DM-nucleon scattering cross section via the Migdal effect for sub-GeV DM using the S2-only data of PandaX-II and PandaX-4T with improved simulations of the Earth shielding effect. Based on the updated constraints, we show that the Migdal effect induced diurnal modulation of electron events can still be significant in the low energy region, and can be probed by experiments such as PandaX-4T in the near future.

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“…Still empty-handed, physicists are extending their searches to the lighter end of the possible mass range: below 1 GeV. As part of that effort, the team behind the Super-Kamiokande experiment in Japan have now analyzed more than two decades' worth of data to constrain the properties of dark matter particles with masses between 1 and 300 MeV [1].…”

Section: By Marric Stephensmentioning

confidence: 99%